September 17, 2007: Dr. Margarita Karovska (Harvard-Smithsonian Center for Astrophysics) and
collaborators are performing a comprehensive study of the Mira AB interacting system, using the WFPC2 camera on the Hubble Space Telescope. Mira AB is composed of the prototype Mira variable omi Cet and its companion VZ Cet, separated by about 0.5 arcsecond. As part of this project they plan to obtain a large number of high-angular resolution images at wavelengths ranging from UV to optical. The main objectives of the HST/WFPC2 observations are:
Mira variables are the longest-observed class of stars for which we have long-term quantitative data that allow us to study their behavior over centuries-long periods of time. Fortunately for us, they're also easy to observe and monitor, having some of the largest amplitudes of all variables, and hundreds of them are bright enough that they're within reach of astronomers with modest telescopes.
The following form will allow you to generate a customized copy of the AAVSO Bulletin suited to your needs. You may select stars from a given constellation, range of Right Ascension and/or Declination, or simply type in a list of stars you would like returned. You may also customize the page that's output by color-coding the months depending upon the brightness of the star, and also limit output to a single month. Leaving all options blank will give you the complete list of stars in this issue of the Bulletin with no color added to the table.
STARS IN NEED OF OBSERVATIONS
AAVSO BULLETIN 73: Predicted Maxima and Minima of Long Period Variables for 2010
The stars listed below need additional observations. Please be aware that many of these
stars are difficult to observe, and should be observed only by experienced observers.
Please note that the symbol % after a star name indicates the star has fair to excellent
CCDV or multicolor photometry but still needs visual observations. Because all of the